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.. _cosmology-calculator:
Cosmology Calculator
====================
The cosmology calculator can be used to calculate cosmological distances and
times given a set of cosmological parameters. A cosmological dataset, ``ds``,
will automatically have a cosmology calculator configured with the correct
parameters associated with it as ``ds.cosmology``. A standalone
:class:`~yt.utilities.cosmology.Cosmology` calculator object can be created
in the following way:
.. code-block:: python
from yt.utilities.cosmology import Cosmology
co = Cosmology(
hubble_constant=0.7,
omega_matter=0.3,
omega_lambda=0.7,
omega_curvature=0.0,
omega_radiation=0.0,
)
Once created, various distance calculations as well as conversions between
redshift and time are available:
.. notebook-cell::
from yt.utilities.cosmology import Cosmology
co = Cosmology()
# Hubble distance (c / h)
print("hubble distance", co.hubble_distance())
# distance from z = 0 to 0.5
print("comoving radial distance", co.comoving_radial_distance(0, 0.5).in_units("Mpccm/h"))
# transverse distance
print("transverse distance", co.comoving_transverse_distance(0, 0.5).in_units("Mpccm/h"))
# comoving volume
print("comoving volume", co.comoving_volume(0, 0.5).in_units("Gpccm**3"))
# angular diameter distance
print("angular diameter distance", co.angular_diameter_distance(0, 0.5).in_units("Mpc/h"))
# angular scale
print("angular scale", co.angular_scale(0, 0.5).in_units("Mpc/degree"))
# luminosity distance
print("luminosity distance", co.luminosity_distance(0, 0.5).in_units("Mpc/h"))
# time between two redshifts
print("lookback time", co.lookback_time(0, 0.5).in_units("Gyr"))
# critical density
print("critical density", co.critical_density(0))
# Hubble parameter at a given redshift
print("hubble parameter", co.hubble_parameter(0).in_units("km/s/Mpc"))
# convert time after Big Bang to redshift
my_t = co.quan(8, "Gyr")
print("z from t", co.z_from_t(my_t))
# convert redshift to time after Big Bang
print("t from z", co.t_from_z(0.5).in_units("Gyr"))
.. warning::
Cosmological distance calculations return values that are either
in the comoving or proper frame, depending on the specific quantity. For
simplicity, the proper and comoving frames are set equal to each other
within the cosmology calculator. This means that for some distance value,
x, x.to("Mpc") and x.to("Mpccm") will be the same. The user should take
care to understand which reference frame is correct for the given calculation.
The helper functions, ``co.quan``
and ``co.arr`` exist to create unitful ``YTQuantities`` and ``YTArray`` with the
unit registry of the cosmology calculator. For more information on the usage
and meaning of each calculation, consult the reference documentation at
:ref:`cosmology-calculator-ref`.
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